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Thermal non-line-of-sight imaging from specular and diffuse reflections

Masaki Kaga, Takahiro Kushida, Tsuyoshi Takatani, Kenichiro Tanaka, Takuya Funatomi, Yasuhiro Mukaigawa
2019 IPSJ Transactions on Computer Vision and Applications  
This paper presents a non-line-of-sight technique to estimate the position and temperature of an occluded object from a camera via reflection on a wall.  ...  the wall by using a conventional thermal camera.  ...  Non-line-of-sight (NLOS) imaging is a technique to deal with the problem, which reconstructs the position, shape, and reflectance of the hidden objects from indirect light paths.  ... 
doi:10.1186/s41074-019-0060-4 fatcat:rkszpk7r3vdhxau6c7qhpuwd4u

Relationships between Galactic Radio Continuum and Hα Emission

L. E. Cram, A. J. Green, D. C.-J. Bock
1998 Publications Astronomical Society of Australia  
, including the relative importance of thermal and non-thermal radio emission and the degree of optical obscuration.  ...  On the other hand, radio continuum radiation due to non-thermal synchrotron emission is formed by species and processes not involved in thermal emission.  ...  The total brightness of thermal radiation along a specified line of sight is the integral of this expression, provided that the line of sight is optically thin.  ... 
doi:10.1071/as98064 fatcat:qaa3wd7movcpdfb5uvmx63gdfu

Ionized Gas in the SgrA Complex - VLA Observations of H168alpha and H270alpha Recombination Lines [article]

K.R. Anantharamaiah, A. Pedlar, W.M. Goss
1999 arXiv   pre-print
Radio recombination lines at a wavelength of 20 cm reveals the presence of an extended component of ionized gas of lower density in the Sgr A complex.  ...  This component extends well beyond the thermal 'mini-spiral' SgrA-West, which seem to be embedded in it.  ...  If we assume that ionized gas with the same properties extends over whole of SgrA East (i.e. about 4 arminutes), then the total ionized mass is ∼ 8 × 10 4 M ⊙ .  ... 
arXiv:astro-ph/9903072v1 fatcat:t73bajkksbgorlsw3nhj7onigi

Multi-Wavelength Observation Results of the C5.6 Limb Flare of 1 August 2003

Hui Li, Jianqi You, Qiusheng Du, Xingfeng Yu
2004 Solar Physics  
The RHESSI observations give a thermal energy spectrum for this flare, and two thermal sources and no non-thermal source are found in the reconstructed RHESSI images.  ...  The significant increases of the Doppler widths of these lines in the impulsive phase reflect quick heating of the chromosphere, and rapid rising and expanding of the flare loop.  ...  SOHO is a project of international cooperation between ESA and NASA.  ... 
doi:10.1007/s11207-004-3260-7 fatcat:xypaqn6tdfc6bij54znd2uhihu

Dust Temperatures and Opacities in the Central Parsec of the Galactic Center Modeled from Analysis of Multi-wavelength Mid-infrared Images

F. Varosi, D. Gezari, E. Dwek, C. Telesco
2015 Proceedings of the International Astronomical Union  
We have analyzed multi-wavelength mid-infrared images of the central parsec of the Galactic Center using a two-temperature line-of-sight (LOS) radiative transfer model at each pixel of the images, giving  ...  The data consists of images at nine wavelengths in the mid-infrared (N-band and Q-band) from the Thermal Region Camera and Spectrograph (T-ReCS) instrument operating at the Gemini South Observatory.  ...  We have analyzed multi-wavelength mid-infrared images of the central parsec of the Galactic Center using a two-temperature line-of-sight (LOS) radiative transfer model at each pixel of the images, giving  ... 
doi:10.1017/s1743921316008413 fatcat:ghkfjvvfergvnd5augrohp5g4i

Alfvén Wave Turbulence as a Coronal Heating Mechanism: Simultaneously Predicting the Heating Rate and the Wave-induced Emission Line Broadening

R. Oran, E. Landi, B. van der Holst, I. V. Sokolov, T. I. Gombosi
2017 Astrophysical Journal  
Combining 3D model results with the CHIANTI atomic database, we were able to create synthetic line-of-sight spectra which include the effects of emission line broadening due to both thermal and wave-related  ...  To the best of our knowledge this is the first time a global model is used to obtain synthetic non-thermal line broadening.  ...  Analysis of radiative processes was made possible through the use of the CHIANTI atomic database.  ... 
doi:10.3847/1538-4357/aa7fec fatcat:ngtesz2nv5euxdjg763b7mymta

Alfvén Wave Turbulence as a Coronal Heating Mechanism: Simultaneously Predicting the Heating Rate and the Wave-Induced Emission Line Broadening [article]

R. Oran, E. Landi, B. van der Holst, I. V. Sokolov, T. I. Gombosi
2014 arXiv   pre-print
Combining 3D model results with the CHIANTI atomic database, we were able to create synthetic line-of-sight spectra which include the effects of emission line broadening due to both thermal and wave-related  ...  To the best of our knowledge this is the first time a global model is used to obtain synthetic non-thermal line broadening.  ...  Analysis of radiative processes was made possible through the use of the CHIANTI atomic database.  ... 
arXiv:1401.0565v1 fatcat:brvji2mzozffhp3nqb7henwd3e

Probing Interstellar Turbulence in the Warm Ionized Medium using Emission Lines [article]

S. L. Tufte, R. J. Reynolds, L. M. Haffner
1998 arXiv   pre-print
many lines of sight this component dominates.  ...  By measuring the widths of the H-alpha line and an emission line from a heavier atom (e.g. the [S II] 6716 line), one can separate the thermal and non-thermal contributions to the line width.  ...  Non-thermal Line Broadening in the WIM The measured widths of the Hα line from the WIM range from 15 to 50 km s −1 and result from thermal and non-thermal broadening mechanisms.  ... 
arXiv:astro-ph/9811313v1 fatcat:x3vywoebl5elxnq7473wvvhefa

The 5th International Conference on Radiotherapy Gel Dosimetry (DOSGEL 2008)

Thomas G Maris, Evangelos Pappas
2009 Journal of Physics, Conference Series  
Non-thermal velocity measurements of the solar atmosphere, particularly from UV and X-ray emission lines have demonstrated over the decades that this parameter is important in understanding the triggering  ...  Three of the flares were eruptive and one was confined. In all events, pre-flare enhancement in non-thermal velocity at the base of the active region and its surroundings has been found.  ...  Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/ JAXA. This team mainly consists of scientists from institutes in the partner countries.  ... 
doi:10.1088/1742-6596/164/1/011001 fatcat:q7gzj3podzfxjjoms3xz2ymn2u

THE LOCATION OF NON-THERMAL VELOCITY IN THE EARLY PHASES OF LARGE FLARES—REVEALING PRE-ERUPTION FLUX ROPES

Louise K. Harra, Sarah Matthews, J. L. Culhane, Mark C. M. Cheung, Eduard P. Kontar, Hirohisa Hara
2013 Astrophysical Journal  
Non-thermal velocity measurements of the solar atmosphere, particularly from UV and X-ray emission lines have demonstrated over the decades that this parameter is important in understanding the triggering  ...  Three of the flares were eruptive and one was confined. In all events, pre-flare enhancement in non-thermal velocity at the base of the active region and its surroundings has been found.  ...  Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/ JAXA. This team mainly consists of scientists from institutes in the partner countries.  ... 
doi:10.1088/0004-637x/774/2/122 fatcat:4jz6xg63bnb4zcvbsdtxcqifoa

A new complex variable element-free Galerkin method for two-dimensional potential problems

Yu-Min Cheng, Jian-Fei Wang, Fu-Nong Bai
2012 Chinese Physics B  
Non-thermal velocity measurements of the solar atmosphere, particularly from UV and X-ray emission lines have demonstrated over the decades that this parameter is important in understanding the triggering  ...  Three of the flares were eruptive and one was confined. In all events, pre-flare enhancement in non-thermal velocity at the base of the active region and its surroundings has been found.  ...  Scientific operation of the Hinode mission is conducted by the Hinode science team organized at ISAS/ JAXA. This team mainly consists of scientists from institutes in the partner countries.  ... 
doi:10.1088/1674-1056/21/9/090203 fatcat:d6pzrghahngjrho26iernahofq

A solar tornado observed by EIS

P. J. Levens, N. Labrosse, L. Fletcher, B. Schmieder
2015 Astronomy and Astrophysics  
Using Gaussian fitting to fit and de-blend the spectral lines seen by EIS, we calculated line-of-sight velocities and non-thermal line widths.  ...  Non-thermal line widths show broader profiles at the tornado location when compared to the surrounding corona.  ...  CHIANTI is a collaborative project involving George Mason University, the University of Michigan (USA) and the University of Cambridge (UK).  ... 
doi:10.1051/0004-6361/201425586 fatcat:vme5ni736bdipen4iiswbx3pja

SPECTROSCOPIC ANALYSIS OF INTERACTION BETWEEN AN EXTREME-ULTRAVIOLET IMAGING TELESCOPE WAVE AND A CORONAL UPFLOW REGION

F. Chen, M. D. Ding, P. F. Chen, L. K. Harra
2011 Astrophysical Journal  
A more interesting finding is that the upflow and non-thermal velocities in the upflow region are suddenly diminished after the transit of the wave front.  ...  This implies a significant change of magnetic field orientation when the wave passed. As the lines in the upflow region are redirected, the velocity along the line of sight is diminished as a result.  ...  Since one of the main causes of the non-thermal velocity is the multiplicity of line of sight velocities, the sudden diminishing of the non-thermal velocity could therefore be explained.  ... 
doi:10.1088/0004-637x/740/2/116 fatcat:d5yizbotkfhnphrkpyprhe4z2e

PLASMA DYNAMICS ABOVE SOLAR FLARE SOFT X-RAY LOOP TOPS

G. A. Doschek, D. E. McKenzie, H. P. Warren
2014 Astrophysical Journal  
Non-thermal motions that may be due to turbulence or multiple flow regions along the line of sight are extracted from the line profiles.  ...  The non-thermal motions measured along the line of sight, as well as their apparent increase with height, are supported by Solar Dynamics Observatory Atmospheric Imaging Assembly measurements of turbulent  ...  We find this coincidence to be strong support for the interpretation of the non-thermal broadening as being due to turbulence, rather than waves or bulk flows along the line of sight.  ... 
doi:10.1088/0004-637x/788/1/26 fatcat:oscvdpplqrdyjdryit7alemf4u

Cyg OB2 #5: When three stars are just not enough [article]

M. Kennedy, S.M. Dougherty, P.M. Williams, A. Fink
2010 arXiv   pre-print
The radio emission consists of a primary component associated with the binary, and a non-thermal source (NE), 0.8" to the NE.  ...  The variable radio emission from the primary has a period of 6.7+/-0.3 years which is described by a simple model of a non-thermal source orbiting within the stellar wind envelope of the binary.  ...  The line-of-sight opacity is dependent on the geometry of the line-of-sight to the non-thermal emission. Here, the case of a non-thermal source in a 6.7-yr orbit about the binary is considered.  ... 
arXiv:1011.0777v1 fatcat:7y7a4hthw5h4ppd2vpmv73k2ua
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